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Just uploading a grayscale version of this so I can keep all the observations from this proposition organized better. The color version is here: flic.kr/p/2dqvScX
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 37.73° clockwise from up.
Sundays early autumn tour at Gimborn near Marienheide. Can you spot the two pieces I'm currently testing?
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Sonntags Frühherbst Tour bei Gimborn nahe Marienheide. Könnt ihr die zwei Teile ausmachen, die ich gerade teste?
Mountain due east of Las Vegas on the border of Lake Mead draws in the early red shifted light of morning.
Draco is a constellation in the far northern sky. Its name is Latin for dragon. It was one of the 48 constellations listed by the 2nd century astronomer Ptolemy, and remains one of the 88 modern constellations today. The north pole of the ecliptic is in Draco. Draco is circumpolar (that is, never setting), and can be seen all year from northern latitudes.
Thuban (α Draconis) was the northern pole star from 3942 BC, when it moved farther north than Theta Boötis, until 1793 BC. The Egyptian Pyramids were designed to have one side facing north, with an entrance passage geometrically aligned so that Thuban would be visible at night. Due to the effects of precession, it will again be the pole star around the year AD 21000. It is a blue-white giant star of magnitude 3.7, 309 light-years from Earth. The traditional name of Alpha Draconis, Thuban, means "head of the serpent".
There are three stars under magnitude 3 in Draco. The brighter of the three, and the brightest star in Draco, is Gamma Draconis, traditionally called Etamin or Eltanin. It is an orange giant star of magnitude 2.2, 148 light-years from Earth. The aberration of starlight was discovered in 1728 when James Bradley observed Gamma Draconis. Nearby Beta Draconis, traditionally called Rastaban, is a yellow giant star of magnitude 2.8, 362 light-years from Earth. Its name shares a meaning with Thuban, "head of the serpent".[1]Draco also features several interacting galaxies and galaxy clusters. One such massive cluster is Abell 2218, located at a distance of 3 billion light-years (redshift 0.171).
Draco is home to several double stars and binary stars. Eta Draconis (the proper name is Athebyne) is a double star with a yellow-hued primary of magnitude 2.8 and a white-hued secondary of magnitude 8.2 located south of the primary. The two are separated by 4.8 arcseconds. Mu Draconis, traditionally called Alrakis, is a binary star with two white components. Magnitude 5.6 and 5.7, the two components orbit each other every 670 years. The Alrakis system is 88 light-years from Earth. Nu Draconis is a similar binary star with two white components, 100 light-years from Earth. Both components are of magnitude 4.9 and can be distinguished in a small amateur telescope or a pair of binoculars. Omicron Draconis is a double star divisible in small telescopes. The primary is an orange giant of magnitude 4.6, 322 light-years from Earth. The secondary is of magnitude 7.8. Psi Draconis (the proper name is Dziban ) is a binary star divisible in binoculars and small amateur telescopes, 72 light-years from Earth. The primary is a yellow-white star of magnitude 4.6 and the secondary is a yellow star of magnitude 5.8. 16 Draconis and 17 Draconis are part of a triple star 400 light-years from Earth, divisible in medium-sized amateur telescopes. The primary, a blue-white star of magnitude 5.1, is itself a binary with components of magnitude 5.4 and 6.5. The secondary is of magnitude 5.5 and the system is 400 light-years away.[1] 20 Draconis is a binary star with a white-hued primary of magnitude 7.1 and a yellow-hued secondary of magnitude 7.3 located east-northeast of the primary. The two are separated by 1.2 arcseconds at their maximum and have an orbital period of 420 years. As of 2012, the two components are approaching their maximum separation.[4] 39 Draconis is a triple star 188 light-years from Earth, divisible in small amateur telescopes. The primary is a blue star of magnitude 5.0, the secondary is a yellow star of magnitude 7.4, and the tertiary is a star of magnitude 8.0; the tertiary appears to be a close companion to the primary. 40 Draconis and 41 Draconis are a binary star divisible in small telescopes. The two orange dwarf stars are 170 light-years from Earth and are of magnitude 5.7 and 6.1.
R Draconis is a red Mira-type variable star with a period of about 8 months. Its average minimum magnitude is approximately 12.4, and its average maximum magnitude is approximately 7.6. It was discovered to be a variable star by Hans Geelmuyden in 1876.
The constellation contains the star recently named Kepler-10, which has been confirmed to be orbited by Kepler-10b, the smallest rocky Earth-sized planet yet detected outside of the Solar System.
One of deep-sky objects in Draco is the Cat's Eye Nebula (NGC 6543), a planetary nebula approximately 3,000 light-years away that was discovered by English astronomer William Herschel in 1786. It is 9th magnitude and was named for its appearance in the Hubble Space Telescope, though it appears as a fuzzy blue-green disk in an amateur telescope.[1] NGC 6543 has a very complex shape due to gravitational interactions between the components of the multiple star at its center, the progenitor of the nebula approximately 1,000 years ago.[6] It is located 9.6 arcminutes away from the north ecliptic pole to the west-northwest. It is also related to IC 4677, a nebula that appears as a bar 1.8 arcminutes to the west of the Cat's Eye nebula. In long-term exposures, IC 4677 appears as a portion of a ring surrounding the planetary nebula.
There are several faint galaxies in Draco, one of which is the lenticular galaxy NGC 5866 (sometimes considered to be Messier Object 102) that bears its name to a small group that also includes the spiral galaxies NGC 5879 and NGC 5907. Another is the Draco Dwarf Galaxy, one of the least luminous galaxies with an absolute magnitude of −8.6 and a diameter of only about 3,500 light years, discovered by Albert G. Wilson of Lowell Observatory in 1954. Another dwarf galaxy found in this constellation is PGC 39058.
PGC 39058, a dwarf galaxy found within the Draco constellation – picture taken by ESA/Hubble & NASA.
Draco also features several interacting galaxies and galaxy clusters. One such massive cluster is Abell 2218, located at a distance of 3 billion light-years (redshift 0.171). It acts as a gravitational lens for even more distant background galaxies, allowing astronomers to study those galaxies as well as Abell 2218 itself; more specifically, the lensing effect allows astronomers to confirm the cluster's mass as determined by x-ray emissions. One of the most well-known interacting galaxies is Arp 188, also called the "Tadpole Galaxy". Named for its appearance, which features a "tail" of stars 280,000 light-years long, the Tadpole Galaxy is at a distance of 420 million light-years (redshift 0.0314). The tail of stars drawn off the Tadpole Galaxy appears blue because the gravitational interaction disturbed clouds of gas and sparked star formation.
Q1634+706 is a quasar that holds the distinction of being the most distant object usually visible in an amateur telescope. At magnitude 14.4, it appears star-like, though it is at a distance of 12.9 billion light-years. The light of Q1634+706 has taken 8.6 billion years to reach Earth, a discrepancy attributable to the expansion of the universe.
Located in the northern celestial hemisphere, Abell 1703 is composed of over one hundred different galaxies that act as a powerful cosmic telescope, or gravitational lens. The gravitational lens produced by the massive galaxy cluster in the foreground (the yellow mostly elliptical galaxies scattered across the image) bends the light rays in a way that can stretch the images and so amplify the brightness of the light rays from more distant galaxies. In the process it distorts their shapes and produces multiple banana-shaped images of the original galaxies. The result is the stunning image seen here - a view deeper into the Universe than possible with current technology alone. Abell 1703 is located at 3 billion light-years from the Earth (redshift 0.26).
NGC 7479, Caldwell 44, Pegasus, Propeller Galaxy
NGC7479 is a distorted barred spiral galaxy in the constellation of Pegasus, discovered by W. Herschel in 1784. With apparent diameter of 4.4 arcmin, and apparent magnitude of 10.85 (V), visual observation calls for large apertures. However, its basic structures are evident photographically with modest telescopes. From its measurable properties we can derive light travel distance (lookback time) of 110 million light years, redshift recession velocity of 2,379 km/s, actual diameter of 140,000 ly, and absolute magnitude of -21.83 (V), approximately 1.5 times as bright as the Milky Way. NGC7479 has an active galactic nucleus (AGN) which is 8.5 times brighter in the near IR (z filter) than in the visible band, and which emits narrow spectral lines of weakly ionized elements. These characteristics classify it as a Seyfert 2 and a LINER galaxy. It is powered by an actively accreting central supermassive black hole (SMBH) obscured by a large, dense cloud of light-absobing gas and dust. The nucleus is also active at radio frequencies, suggesting the SMBH has polar jets emitting synchrotron radiation. Bright blue floccules in the spiral arms and even within the bar are OB Associations, or vast clusters of recently formed blue giant stars which emit most of their energy in the ultraviolet band. NGC7479 is an isolated field galaxy with no nearby neighbors. Starburst activity, several stellar streams, and gravitational distortion in the W spiral arm are thought to have been caused by a merger with one or more dwarf satellite galaxies between 300 and 100 million years ago.
As the annotated image illustrates, different spectral bands reveal different details within a galaxy. In the ultraviolet band (GALEX), the most prominent features are OB associations, starburst regions, and reflection nebulae. The compact, round UV signal overlapping the N arm of the bar may be the remnant nucleus of a merged dwarf galaxy. The NGC7479 nucleus is not prominent because it is surrounded by a thick layer of gas and dust which absorb and scatter predominantly UV light. However, the brightest feature on the infrared (2MASS) image of the galaxy is precisely the main galactic nucleus with a central SMBH, because longer wavelengths are less obsured. The bulge and the bar are also distinctive due to the presence of ancient cool and red Population II stars. Radio frequency imaging of the galaxy reveals the presence of a bright jet-like feature, centered on the nucleus, and extending through the bar about 20,000 light years in the N and in the S direction. The jet's spiral morphology mildly curves in the direction opposite to that of the stellar and gaseous spiral arms, suggesting that the two structures may be counter-rotating. Jet bending can be caused by precession of the central SMBH accretion disk, by the presence of a binary central SMBH, and/or an off center merger with another galaxy. Based on the rate of expansion and the maximum distance from the nucleus, the jet is felt to be less than 10 million years old.
A large galaxy cluster is visible in the remote background at an estimated light travel distance of 1.5 to 2 billion light years. Only two of these have assigned identifiers. Their measurable and derived properties are listed in the chart on the annotated image.
Image details:
-Remote Takahashi TOA 150 x 1105 mm, Paramount GT GEM,
-OSC 34 x 300 sec, 2x drizzle, 50% linear crop,
-Software: DSS, XnView, StarNet++ v2, StarTools v1.3 and 1.7, Cosmological Calculator v3
it might be hard for people these days to imagine that the was a time before editing tools of the digital kind all around us... this is me as a youngling a picture taken of me holding my own head in my hand which I used as a Christmas card and sent to fiends and friends alike...
this is the original photo without the Christmas greetings... well the original photo of my hand since the pic of my mug is another photo taken by me, a kind of double-self-portrait...
Peace and Noise!
this is a pic from some of my experimenting with my old analog Zenit systematic camera, with long time shutter exposure and a heavy light source you could become impish, goblin-like and monstrous, great fun for a silly young chap like me :) hooked on the role-playing fantasy aesthetics ;)
Peace and Noise!
/ MushroomBrain
A scant dwarf galaxy imaged a few days ago by Hubble. There isn't a whole lot to see here beyond the central smudge and the rather impressive area of star formation along the lower edge of the composition. It is interesting that all of the older, dimmer stars seem to come together in a smooth central region, while brighter, younger, individually resolved stars lie in the outer regions, much like a larger spiral galaxy.
This image marks the first moment I am fully caught up on all of the observations in this proposal. I can now simply process them as they come along instead of madly trying to catch up only to fall behind as each new image comes down.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 47.02° counter-clockwise from up.
My J.Guillem Orient in front of the Junior University in Wuppertal.
Current spec:
J.Guillem Orient frame, J.Guillem Titanium seat post, SRAM red eTap HRD group, Quarq DZero Powermeter, Brooks Cambium C15 carved saddle, redshift sports Shockstop Stem, Profile Design T1+ aerobars, DT Swiss ERC 1400 Spline 47 wheels, Vittoria Corsa G+ tires.
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Mein J.Guillem Orient vor der Junior Uni in Wuppertal.
Aktuelle Konfiguration:
J.Guillem Orient frame, J.Guillem Titan-Sattelstütze, SRAM red eTap HRD Gruppe, Quarq DZero Leistungsmesser, Brooks Cambium C15 carved Sattel, redshift sports Shockstop Stem, Profile Design T1+ aerobars, DT Swiss ERC 1400 Spline 47 Laufräder, Vittoria Corsa G+ Reifen.
NGC 5364 (NGC 5317) and NGC 5363 Galaxy Group,Virgo
NGC 5364, also catalogued as NGC 5317, is a "grand-design" spiral galaxy discovered by William Herschel in 1786. Its morphological classification of SA(rs)bc pec indicates an incomplete ring structure, loosely wound spiral arms, and a peculiar asymmetry of the galactic bulge and the spiral arms which is probably due to gravitational perturbation by its neighbors. The most likely cause is the nearby lenticular galaxy NGC 5360, although some sources suggest that the more distant NGC 5363 also shows evidence of gravitational interaction. Based on its redshift and apparent size and magnitude, NGC 5364 is about 57.4 million light years distant, and receding at 1,239 km/s due to the expansion of the Universe. It is approximately 93,000 LY in diameter, and half as bright as the Milky Way. Light blue floccules in the spiral arms are OB Associations, or immense clusters of large, very hot young stars. Hubble images of the galaxy also show numerous regions of hydrogen gas partially ionised by ultraviolet light from recently formed stars.
The other major galaxy in the image is NGC 5363, also discovered by William Herschel in 1784. As a fairly featureless lenticular galaxy, with a well developed nuclear bulge and a diffuse galactic disk, it is far less spectacular in the visible band than its grand-design spiral companion. However, in the infrared band, the galaxy displays two prominent lanes of cold dust which still retain evidence of a spiral structure and a central bar. The total mass of interstellar dust is about 100 times greater than expected from the total mass lost by evolved stars, which suggests an external origin. The detection of density shells within the galaxy as evidence of recent mergers confirms the hypothesis that the excess interstellar dust was acquired through accretion. Further, ultraviolet studies reveal the presence of young, hot stars born during star formation activity caused by a recent merger. Spectroscopic studies of the central region show evidence of an active galactic nucleus (AGN) of the LINER type, powered by the accretion disk of a central supermassive black hole (SMBH) with a mass of 375 million solar. The AGN is also a source of radio waves, indicating the precence of polar jets emanating from the central SMBH, generating synchrotron radiation. Thus, when studied throughout the electromagnetic spectrum, this apparently featureless galaxy tells a fascinating story. Based on measurable properties (redshift, apparent magnitude, and angular size), NGC 5363 is about 90,000 LY in diameter, and one third as bright as the Milky Way (much of its visible light is extincted by the dust). It lies at a distance of 57 million LY, receding at 1,129 km/s due to the expansion of the Universe. It is approximately 5 million LY distant from its spiral companion, NGC 5364, so it does not appear likely that either is tidaly deforming the other at present, though they are members of the same gravitationally bound galaxy cluster.
The other members within the photograph belonging to the NGC 5364 galaxy group are marked in light blue color on the annotated image, and their physical properties are described on the attached chart. The group belongs to the Virgo III Galaxy Group, which is itself the E part of the large Virgo Galaxy Cluster.
www.atlasoftheuniverse.com/galgrps/viriii.html
In the backround lie more remote galaxies at distances between 250 million and 1.5 billion LY. These are marked in green and yellow color on the annotated image, depending on their redshift. Included also are four quasars QSOs). The most distant of these is WISEA J135345.93+051305.4. Its redshift of 3.400 indicates that the light we are presently recording travelled for 11.8 billion years to reach us (lookback time, or light travel distance). When the light was emitted, the quasar was about 16,000 times brighter than the Milky Way, and was receding from the future location of our galaxy at 270,343 km/sec (redshift, apparent, or relativistic recession velocity). In the present epoch, its (comoving = proper) distance is around 22.4 billion LY, and it is receding at the superluminal proper recession velocity of 483,700 km/s. The quasar is presently located well beyond the cosmic event horizon, and the photons it is presently emitting can never reach us. It can be calculated that 99.73% of the light originally emitted was lost to "cosmological extinction", or literally diluted by the expansion of space through which it travelled.
Image Details:
-Remote Takahashi TOA 150 x 1105mm, Paramount GT GEM
-29 x 300 sec OSC, 15% and 25% area crop
-Software:
DSS, XnView, StarNet++, StarTools v 1.3 and 1.7,
Extragalactic Cosmological Calculator 2
A brand new pinhole camera from Reality So Subtle (35r). It has 2 pinholes, one on the front and one on the back, The back one is used dfor shooting "redscale". © www.johnfar.com
Just uploading a grayscale version of this so I can keep all the observations from this proposition organized better. The color version is here: flic.kr/p/2dDdQq5
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is up.
United Arab Emirates Air Force, Sikorsky UH-60L Blackhawk, msn 42361, reg 2621. Seen at Dubai Airshow 2021 held at Al Maktoum DWC / OMDW. carrying two Alta Redshift electric motorbikes (one each side) two deploy a Silent Special Ops team or take your cousins for a desert joy trip.
NGC 3184 (NGC 3180), (Little Pinwheel Galaxy), NGC 3179, Ursa Major
Image Details:
-TSAPO100Q astrograph, Sigma APO 1.4x tele-extender (100 x 812 mm)
- Ioptron IEQ30pro mount, Orion 60mm F/4 SSAGpro autoguider
-Canon T3i camera, no filters
-20 x 240 sec exposures, iso 1600, 30 darks, 30 bias, 2x drizzle, 25% crop
-Software: PHD2, DSS, XnView, StarNet++, StarTools v 1.3 and 1.7
-Limiting magnitude on the original is better than 18.5.
NGC 3184 (NGC 3180), (Little Pinwheel Galaxy), NGC 3179, Ursa Major
NGC 3184 is a face-on mixed barred-nonbarred spiral galaxy with morphological classification SABc. NED database lists its apparent magnitude in the visible band between 13.5 and 11.49, which is the most recent (1977), and will be adopted here, although it appears at least 1 magnitude brighter on my photograph. Its mean redshift-independent distance is 12.268 Mpc, or 40 Mly. Its redshift-based (Hubble Flow) distance calculated in the chart below is 27.35 million light years, and recession velocity 590 km/sec. Based on its angular size of 8.5 arcmin, the galaxy is about 67,500 ly in diameter. Its calculated absolute magnitude of only -18.14 is probably too low, and should be updated with more reliable photometric data. The galaxy has a small, bright nucleus and long spiral arms rendered prominently blue by large numbers of hot, young stars and OB associations. Due to an error in the New General Catalog, this galaxy is also listed as NGC 3180. The galaxy is notable for a high abundance of heavy elements, making it suitable for rocky planets and interesting exobiology. From its perspective, our Galaxy would appear about twice as large in diameter, and much brighter. Photography indicates the presence of several large star-forming HII regions. The most prominent one is designted as NGC 3181. The annotated image below indicates the position of an ultra-luminous X-ray source (ULX), possibly indicating the presence of an intermediate-mass black hole. Such objects can be associated with bright transient optical signals lasting several days.
www.cloudynights.com/articles/cat/articles/transient-opti...
About 25 arcmin to the south is NGC 3179, a magnitude 13.7 (g) galaxy, 2 arcmin in apparent size. It seems to be a giant spiral galaxy, 326 million LY distant, and about 70% larger in diameter and brighter than the Milky Way.
The most remote recorded object is quasar (QSO) [VV96] J101732.7+410722. Based on its redshift and apparent magnitude, it can be calculated that the photons presently reaching us were emitted 6.2 billion years ago, long before the formation of our Solar system. It is about 83 times brighter than the entire Milky Way galaxy, and is receding due to the expansion of the universe at nearly half the speed of light.
Just uploading a grayscale version of this so I can keep all the observations from this proposition organized better. The color version is here: flic.kr/p/T68ekd
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 8.42° clockwise from up.
The Redshift Star Fighter is always guarded by a pair of elite green soldiers.
While docked the ship is charged from power harnessed from a subterranean volcanic fissure.
NGC 2146 is a disrupted barred spiral galaxy in the constellation of Camelopardalis. It was discovered in 1876 by German astronomer Friedrich Winnecke, who was known for his work on comets, asteroids, and double stars. The galaxy is classified as SB(s)ab pec, indicating a barred spiral galaxy with tightly wound arms, and no ring around the central bulge. The "pec" descriptor refers to the "peculiar" appearance of the spiral arms, one of which is markedly stretched and inclined to the galactic plane by nearly 45*. Very high star formation rate (SFR) and densities within both spiral arms resembling large stellar trails suggest the galaxy recently merged with one or two substantial dwarf satellites, and is presently reforming into a larger object. Some sources suggest that NGC 2146 may have interacted with a nearby small galaxy, NGC 2146a, however that seems unlikely because the small galaxy's spiral structure appears quite well preserved. Aside from its disrupted aspect and starburst activity, NGC 2146 is also distinctive due to its conspicuous dust lanes extending across the background glow of the galactic core. Spectroscopy of the central region reveals widening of spectral lines. This indicates a high velocity dispersion of the stars in the nucleus due to the presence of a central supermassive black hole (SMBH). Absence of an active galactic nucleus means thet the central SMBH is not presently accreting matter.
Assuming its measured redshift of 0.00298 is caused exclusively by the expansion of space (Hubble Flow), NGC 2146 would lie at a distance of 41.3 Mly. However, the median value of 16 redshift-independent distance measurements is 17.40 Mpc, or 56.72 Mly. The two distance estimates differ because the measured redshift actually results from the combined motion due to Hubble Flow and the object's "peculiar velocity" through space. When available in a statistically valid number of measurements, redshift-independent estimates are generally regarded as more accurate for nearby galaxies, closer than approximately 140 Mly. From the apparent magnitude and angular size, accepting the distance of 56.72 Mly, we can derive the galaxy's actual diameter of 97,000 ly and absolute magnitude of -20.64. NGC 2146 is some 20-30% smaller, and about 15% less bright than the Milky Way.
Chandra CXC HIPS X-ray sky survey (SIMBAD) shows numerous X-ray sources within the NGC 2146 core, in the spiral arms, and in its halo. While it is possible that some of the sources may be local to the Milky Way, clustering of the sources around NGC 2146 suggests that most are of extragalactic origin.
The most common mechanism for X-ray emission in astronomical objects involves very hot ionized gases at temperatures of millions to hundreds of millions Kelvin (K). Stellar coronas, especially in young blue giants, emit X-rays, though they are regarded as relatively weak sources. Stronger emissions come from "X-ray binaries", "cataclysmic variable stars", supernova remnants, and hot gas clouds around stellar nurseries. Still stronger localized X-ray emissions are "ultra-luminous X-ray sources" or ULX. These are produced by actively accreting intermediate mass black holes (IMBH), usually identified in galactic disks, and by central supermassive black holes (SMBH) which define "active galactic nuclei" (AGN). By far the most powerful, but very diffuse, sources of X-rays are galaxy clusters.
While it is logical to expect numerous X-ray emissions in an actively merging starburst galaxy with accelerated stellar evolution, NGC 2146 has no identified ultra-luminous X-ray sources and no active galactic nucleus. This does not imply the galaxy contains no intermediate or supermassive black holes, but merely that they are not actively accreting.
On closer inspection, the attached image records a number of small, faint background galaxies, but only two of these have identifiers associated with measurable data. Based on a subjective estimate of their angular size and apparent brightness, the rest probably lie at approximate distances between 1 and 2 Bly. The image also records a single quasar (QSO) at a light travel distance (lookback time) of 9.2 Bly.
The distinctly blue galaxy Gaia DR3 1140883127890416128 may belong to a class of special objects: "Blue Compact Dwarf" galaxies (BCDs), which are field dwarf galaxies with inexplicably high star formation rates. BCDs are rare local versions of the "Faint Blue Galaxies" (FBGs), the most common galaxy type at redshifts between 0.1 and 2, but which are undetectable with small instruments. I estimate the apparent magnitude of this object around 20.5 and angular size at 0.15 arcmin. Unfortunately, no redshift information or color photometry is available in extragalactic databases, and the suspected nature of this galaxy can not be confirmed. For additional details on BCDs and FBGs please see section 32, Dwarf Galaxies, subsections 6 and 7 here:
www.cloudynights.com/articles/cat/articles/basic-extragal...
Image Details:
Remote Takahashi TOA 150x1105 mm
OSC 31x300 sec, 2x drizzle, 40% linear crop, 26x17'
Software:
DSS, XnView, StarNet++ v2, StarTools v1.8
Extragalactic Cosmological Calculator v2
www.cloudynights.com/gallery/image/123530-extragalactic-c...
IC 284 (UGC 2581, PGC 11643 and others) is appears to be a low surface brightness spiral located approximately 123 million light-years away (by redshift) in Perseus.
PGC 11646 (2MASX J03060656+4221569, ZW V 319 and others) is the companion on the right (west). Some sources say this one is behind IC 284.
Luminance – 24x600s – 240 minutes – binned 1x1
RGB – 8x300s – 40 minutes each – binned 2x2
360 minutes total exposure – 6 hours
Imaged December 21st and 22nd, 2022 from Dark Sky New Mexico at Rancho Hidalgo (Animas, New Mexico) with a SBIG STF-8300M on an Astro-Tech AT12RCT at f/8 2432mm.
The 2011 Mobius Wearable Art Runway Show
Friday, May 6 · 7:00pm - 9:00pm - Boston
Created By - Mobius, Inc., Alison Safford, James Ellis Coleman
Program Order and Erratae Mobius Wearable Art 1) Inflatable Metamophosis artist: Charlie Roberts model: Liz Roncka MC talk-introduce the show 2) Liv Chaffee Students -The John Marshall School in Dorchester, MA Deandre Dewhollis, Kyshuari Santana-Everet Jose Pene Rayuana Martin-Milton Xavier Barrietos 3) Marie Ghitman – Two Group Skirts Models: Luke Burrows, Neige Christensen, Sage Dowser, Lisa Hiserodt, Sam Lanier, Jean Martin, Madelyn Medeiros, Jane Messere, Jason Picard, Q, Madelaine Ripley, and Artist 4) Jennifer Hicks - steam punk 5) Amy Keefer (SF) you all know me 6) Katie Pray-zip tease CSW 7) Becky Savitt 8) Ellla Williams- broken Record 9) Ella williams-garbage bag dress 10) Emily D’Angelo – 100% Recyclable 11) Grace Lynn Wilson – Fairy 12) Kaela Cote-Stemmermann - Pagan Sunset 13) Kaela Cote-Stemmermann - Stamp coat, model: Caroline Hickey 14) Mikaela Dalton – Mikaela Dalton – The Devil’s Tune 15) Mikaela Dalton – Untitled (cassette top), Model: Sarah Smith 16) Mikaela Joyce – Bell Jar Dress, Model: Sarah Hertel-Fernandez 17) Mikaela Joyce – Safety Pin Top 18) SeungHye Kim –The Pad Dress 19) Sonya Thorne – Apocalyptic Pieces 1-3, Model: self, Lilia Gaufberg, Zoe Cohen 20) Tess McCabe – Redshift, Model: Molly Harrison 21) William Everston (Representing Seeking Kali) -Sari Scroll for Two, Model: Artist, Karen Everston 22a) Ashley Conchieri – hand Woven and Hand Sewn, Model: Rebecca Chabot 22b) Ashley Conchieri – hand Woven and Hand Sewn, Model: 22c) Ashley Conchieri – hand Woven and Hand Sewn, Model: Monika Plioplyte 23) Julia Dusman – “Tarantula” Necklace 24) Ellen Shea - Little Red Re-Design, Model: Rebecca Woodbury 25) LeeLoo – Fallen post-apocalyptic cyber angel 26) L. Mylott Manning – Insides Out 28) Alyssa Fishenden - Plastic bag and stretch nylon halter dress 29) Robyn Giragosian and Caleb Cole – Pom Prom 30) Rachel Jayson – Dress of sheet music 31) Bethany Haeseler – Fruitloops 32) June Monteiro – “SMARTIE Dress”, Model: Chantal Lima Marquis 33) Jennifer Sherr Designs – Collage and hand painted leather vest, Model: Jess Barnett 34) Stacy A. Scibelli –Sabotage, Models: Meg Kuker, Toni Scibelli 35a) Selina Narov – Silk painted art couture clothing - Model: A. Dorian Rose 35b) Selina Narov – Silk painted art couture clothing - Model: Liz Roncka 35c) Selina Narov – Silk painted art couture clothing - Model: Jennifer Hicks 37) Albert Negredo – RECORDS (word game text) Red dress/Silver bag fabricated by Jane Wang - Model: sara june 38) Stacy A. Scibelli – plated skirt with leather head-piece (Models: tbd) 39) Stephanie Skier – Ephemeral dynamic fiberoptic fiber arts 40) the Bureau of cyberSurreal investigation international webCam Bra for Living I/O Model: Carol Susi 41) Elly Jessop – Glow Dress 42) Raphaela Riepl –Tentacles Flying Teeth, Models: Kira Lorenza Althaler as William Haugh, Florian Maria Sumerauer as Aaron Diskin Finale- 43) Word Game Design Competition Winner: June Monteiro - Model: northern sire
ONLINE BLOG for 2011 Mobius Wearable Art Runway Show: mobius-wearableart2011.blogspot.com/
@ Mobius
725 Harrison Avenue, Suite One
Boston MA 02118
Related Exhibition: A Tool Is A Mirror
NGC 7331, Deer Lick Galaxy Group, Pegasus
NGC 7331, also identified as UGC 12113, PGC 69327, and Caldwell 30, is an unbarred spiral galaxy in the constellation of Pegasus. It is the brightest and largest member of a visual field of galaxies called the Deer Lick Galaxy Group that includes NGC 7325, 7326, 7335, 7336, 7337, 7340, and LEDA 2051985, all of which lie in the background at distances between 290 and 400 million light years. The group was first documented in 1784 by William Herschel.
Based on its measurable features (redshift of 0.002732, apparent magnitude 9.48, and angular size 10.47) we can estimate the following NGC 7331 physical properties: actual diameter 115,000 ly, absolute magnitude -20.86, distance 38 million ly, and recession velocity due to the expansion of the Universe (Hubble flow) 818 km/s. The galaxy is remarkably similar to the Milky Way in size and luminosity, but not strictly speaking in morphology. Although both are spiral galaxies, NGC 7331 is unbarred, while the Milky Way is presently thought to be a barred spiral. Further, NGC 7331 has peculiar features which are most likely due to a merger of large component galaxies in the remote past. Unlike the majority of spiral galaxies, its central bulge and the spiral arm disk rotate in opposite directions, and the central bulge is eccentric toward the N relative to the disk and the stellar halo.
Dwarf galaxy LGG 459 lies in-line with the S edge of the NGC 7331 disk, may be merging with it, and may have gravitationally disrupted the S spiral arm into 4 or 5 branches. Although redshift based distance between the two galaxies is around 4 Mly (assuming redshift is due exclusively to Hubble flow), the actual distance between them could be much smaller if LGG 459 redshift were in part due to "peculiar velocity" through space toward the background, away from the observer.
Spectroscopic analysis of NGC 7331 central region revealed an Hii/LINER active galactic nucleus. Filho et al. (2004) reported core radio luminosity 10 times higher and X-ray emission 10,000 times higher than the Sagittarius A* source in the center of our Galaxy. These studies suggest the presence of an obscured central supermassive black hole of approximately 175 million Solar masses, about 44 times larger than the Milky Way's
arxiv.org/abs/astro-ph/0401593
The distant members of the Deer Lick Group are gravitationally bound to each other and also to the nearby Stephan's Quintet (NGC 7320) Group. Even at the scale of this image, NGC 7337 and 7336 show evidence of tidal interactions. The S side of the field contains a very remote galaxy cluster whose members are annotated with letter G. Unfortunately, none of these galaxies carry identifiers in Simbad or NED extragalactic databases. Comparing their average angular size to that of the Deer Lick Group, I very roughly estimate their distance at 2 billion light years.
Image Details:
-Remote Takahashi TOA 150 x 1105mm
-Paramount GT GEM
-25 x 300 sec subs, OSC, 2x drizzle, 50% linar crop
-Software: DSS, XnView, StarNet++, StarTools v1.3 and 1.7, Cosmological Calculator v2